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\section{Introduction}\label{intro}  \begin{itemize}  \item Why RG/EBs red giants in eclipsing binaries  are useful \item Why we care about understanding when solar-like oscillations can happen  \item Why we think tides and stellar activity affect solar-like oscillations and how we can use models constrained by  observations to investigate \end{itemize}  In the absence of external influences, all evolved giant stars with a convective outer layer should theoretically exhibit solar-like oscillations. However, that is clearly not the case. Approximately one fifth of the known RG/EBs do not show any solar-like oscillation activity at all \citep{gau14}. The fraction of single evolved stars without confirmed binary companions that lack oscillations is unknown. \citet{gau14} proposed that stronger tidal interactions from short-period binaries and increased magnetic activity on spotty giants are linked to absent or damped solar-like oscillations. Now that the oscillating and non-oscillating binaries alike have been well-characterized globally \citep{fra13,raw16,gau16}, we can use the available observations to explore how magnetically active each system is, how stellar evolution likely proceeded, and what role tidal forces have played over time.  In this paper, we perform an in-depth study of 17 18  red giants in eclipsing binaries (hereafter RG/EBs). The sample includes binaries with RG/EBs) which exhibit  a range of orbital periods and solar-like oscillation behavior. Section \ref{review} reviews revisits  thevarious observations, global asteroseismology, atmosphere modeling, and  dynamic eclipsing  binary models that have been based on \emph{Kepler} light curves and radial velocity curves as well as the stellar atmosphere models from high-resolution spectra  used to derive physical parameters for these RG/EBs. We \textbf{verify or update these as appropriate}.  In Section \ref{magnetic}, we quantify each system's magnetic activity by considering photometric variability photometrically  and by performing spectral disentangling to investigate spectral regions sensitive to magnetic activity. spectroscopically.  % go into a little more detail about the methods here  Section \ref{tides} presents 1D stellar evolution models for each system, which are subsequently used to quantify each system's level of tidal forces acting over time. We discuss how magnetic activity, tides, and solar-like oscillations are linked in Section \ref{discuss}, and Section \ref{conclusion} summarizes our results.